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Near-infrared surface brightness fluctuations and optical colours of Magellanic star clusters
This work continues our efforts to calibrate model surface brightnessfluctuation luminosities for the study of unresolved stellarpopulations, through a comparison with the data of Magellanic Cloud starclusters. We present here the relation between absoluteKs-band fluctuation magnitude and (V-I) integrated colour,using data from the Two-Micron All-Sky Survey (2MASS) and the DeepNear-Infrared Southern Sky Survey (DENIS), and from the literature. Wecompare the star cluster sample with the sample of early-type galaxiesand spiral bulges studied by Liu et al. We find that intermediate-age toold star clusters lie along a linear correlation with the same slope,within the errors, of that defined by the galaxies in the versus (V-I)diagram. While the calibration by Liu et al. was determined in thecolour range 1.05 < (V-IC)0 < 1.25, oursholds in the interval . This implies, according to Bruzual-Charlot andMouhcine-Lançon models, that the star clusters and the lateststar formation bursts in the galaxies and bulges constitute an agesequence. At the same time, a slight offset between the galaxies and thestar clusters [the latter are ~0.7 mag fainter than the former at agiven value of (V-I)], caused by the difference in metallicity ofroughly a factor of 2, confirms that the versus (V-I) plane maycontribute to break the age-metallicity degeneracy in intermediate-ageand old stellar populations. The confrontation between models and galaxydata also suggests that galaxies with Ks fluctuationmagnitudes that are brighter than predicted, given their (V-I) colour,might be explained in part by longer lifetimes of thermally pulsingasymptotic giant branch stars. A preliminary comparison between the H2MASS data of the Magellanic star clusters and the sample of 47early-type galaxies and spiral bulges observed by Jensen et al. throughthe F160WHubble Space Telescope filter leads to the same basicconclusions: galaxies and star clusters lie along correlations with thesame slope, and there is a slight offset between the star cluster sampleand the galaxies, caused by their different metallicities. Magellanicstar clusters are single populations, while galaxies are compositestellar systems; moreover, the objects analysed live in differentenvironments. Therefore, our findings mean that the relationship betweenfluctuation magnitudes in the near-infrared, and (V-I) might be a fairlyrobust tool for the study of stellar population ages and metallicities,could provide additional constraints on star formation histories, andaid in the calibration of near-infrared surface brightness fluctuationsfor cosmological distance measurements.
| A Survey of N IV and O IV Features near 3400 Å in O2-O5 Spectra
We have conducted a survey of little-known N IV and O IV multiplets near3400 Å in an extensive sample of well-classified, very earlyO-type spectra. The initial motivation was to search for additionaluseful classification criteria for these types, but an unexpected resultis the high sensitivity of these features to evolutionary CNOprocessing. We have found a useful discriminant between O2 and latertypes in the relative strengths of the O IV multiplets, one of which issubject to selective emission in the hottest spectra; the overallstrengths of these lines also decrease between spectral types O4 and O5.More remarkable, however, are the variations in the N/O ratios amongboth individual stars and clusters. For instance, several O4 If+ spectrahave very large ratios, while main-sequence stars in the Carina Nebulagenerally have smaller values than others of the same spectral types inother regions. These effects correspond to different degrees of mixingof processed material as a function of evolutionary age and initialrotational velocities; the second effect provides significant furtherevidence that very massive stars mix while still on the main sequence.Thus, further analysis of these features will likely provide valuablediagnostics of important evolutionary parameters.
| Infrared Surface Brightness Fluctuations of Magellanic Star Clusters
We present surface brightness fluctuations (SBFs) in the near-IR for 191Magellanic star clusters available in the Second Incremental and All SkyData releases of the Two Micron All Sky Survey (2MASS) and compare themwith SBFs of Fornax Cluster galaxies and with predictions from stellarpopulation models as well. We also construct color-magnitude diagrams(CMDs) for these clusters using the 2MASS Point Source Catalog (PSC).Our goals are twofold. The first is to provide an empirical calibrationof near-IR SBFs, given that existing stellar population synthesis modelsare particularly discrepant in the near-IR. Second, whereas mostprevious SBF studies have focused on old, metal-rich populations, thisis the first application to a system with such a wide range of ages(~106 to more than 1010 yr, i.e., 4 orders ofmagnitude), at the same time that the clusters have a very narrow rangeof metallicities (Z~0.0006-0.01, i.e., 1 order of magnitude only). Sincestellar population synthesis models predict a more complex sensitivityof SBFs to metallicity and age in the near-IR than in the optical, thisanalysis offers a unique way of disentangling the effects of age andmetallicity. We find a satisfactory agreement between models and data.We also confirm that near-IR fluctuations and fluctuation colors aremostly driven by age in the Magellanic cluster populations and that inthis respect they constitute a sequence in which the Fornax Clustergalaxies fit adequately. Fluctuations are powered by red supergiantswith high-mass precursors in young populations and by intermediate-massstars populating the asymptotic giant branch in intermediate-agepopulations. For old populations, the trend with age of both fluctuationmagnitudes and colors can be explained straightforwardly by evolution inthe structure and morphology of the red giant branch. Moreover,fluctuation colors display a tendency to redden with age that can befitted by a straight line. For the star clusters only,(H-Ks)=(0.21+/-0.03)log(age)-(1.29+/-0.22) once galaxies areincluded, (H-Ks)=(0.20+/-0.02)log(age)-(1.25+/-0.16).Finally, we use for the first time a Poissonian approach to establishthe error bars of fluctuation measurements, instead of the customaryMonte Carlo simulations.This research has made use of the NASA/ IPAC Infrared Science Archive,which is operated by the Jet Propulsion Laboratory, California Instituteof Technology, under contract with the National Aeronautics and SpaceAdministration.
| Results of the ESO-SEST Key Programme on CO in the Magellanic Clouds. X. CO emission from star formation regions in LMC and SMC
We present J=1-0 and J=2-1 12CO maps of several star-formingregions in both the Large and the Small Magellanic Cloud, and brieflydiscuss their structure. Many of the detected molecular clouds arerelatively isolated and quite small with dimensions of typically 20 pc.Some larger complexes have been detected, but in all cases the extent ofthe molecular clouds sampled by CO emission is significantly less thanthe extent of the ionized gas of the star-formation region. Very littlediffuse extended CO emission was seen; diffuse CO in between orsurrounding the detected discrete clouds is either very weak or absent.The majority of all LMC lines of sight detected in 13CO hasan isotopic emission ratio I( 12CO)/I( 13CO) ofabout 10, i.e. twice higher than found in Galactic star-formingcomplexes. At the lowest 12CO intensities, the spread ofisotopic emission ratios rapidly increases, low ratios representingrelatively dense and cold molecular gas and high ratios marking COphoto-dissociation at cloud edges.
| OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems
The method developed by Gouliermis et al. (\cite{Gouliermis00}, PaperI), for the detection and classification of stellar systems in the LMC,was used for the identification of stellar associations and openclusters in the central area of the LMC. This method was applied on thestellar catalog produced from a scanned 1.2 m UK Schmidt Telescope Platein U with a field of view almost 6\fdg5 x 6\fdg5, centered on the Bar ofthis galaxy. The survey of the identified systems is presented herefollowed by the results of the investigation on their spatialdistribution and their structural parameters, as were estimatedaccording to our proposed methodology in Paper I. The detected openclusters and stellar associations show to form large filamentarystructures, which are often connected with the loci of HI shells. Thederived mean size of the stellar associations in this survey was foundto agree with the average size found previously by other authors, forstellar associations in different galaxies. This common size of about 80pc might represent a universal scale for the star formation process,whereas the parameter correlations of the detected loose systems supportthe distinction between open clusters and stellar associations.
| Constraints on the Ionization Balance of Hot-Star Winds from FUSE Observations of O Stars in the Large Magellanic Cloud
We present Far Ultraviolet Spectroscopic Explorer (FUSE) spectra for 25O stars in the Large Magellanic Cloud. We analyze wind profiles for theresonance lines from C III, N III, S IV, P V, S VI, and O VI in the FUSErange using a ``Sobolev with exact integration'' method. In addition,the available data from either IUE or the Hubble Space Telescope for theresonance lines of Si IV, C IV, and N V are also modeled. Becauseseveral of the FUSE wind lines are unsaturated, the analysis providesmeaningful optical depths (or equivalently, mass-loss rate timesionization fractions, Mq) as a function of normalized velocity,w=v/v&infy;. Ratios of Mq (which are independent of M)determine the behavior of the relative ionization as a function of w.The results demonstrate that, with the exception of O VI in all starsand S VI in the later stars, the ionization in the winds shifts towardlower ionization stages at higher w (contrary to the expectations of thenebular approximation). This result implies that the dominant productionmechanism for O VI and S VI in the late O stars differs from the otherions. Using the Vink et al. relationship between stellar parameters andmass-loss rate, we convert the measurements into mean ionizationfractions for each ion, 〈qi〉. Because the derived ionfractions never exceed unity, we conclude that the derived values of Mare not too small. However, q(P V), which is expected to be the dominantstage of ionization in some of these winds, is never greater than 0.20.This implies that either the calculated values of M are too large, theassumed abundance of phosphorus is too large, or the winds are stronglyclumped. The implications of each possibility are discussed.Correlations between the mean ion fractions and physical parameters suchas Teff, v&infy;, and the mean wind density,〈ρ〉, are examined. Two clear relationships emerge. First, asexpected, the mean ionization fraction of the lower ions (C III, N III,Si IV, S IV) decreases with increasing Teff. Second, the meanion fraction of S VI in the latest stars and O VI in all stars increaseswith increasing v&infy;. This reaffirms the notion, firstintroduced by Cassinelli & Olson, that O VI is producednonradiatively. Finally, we discuss specific characteristics of threestars, BI 272, BI 208, and Sk -67°166. For BI 272, the ionic speciespresent in its wind suggest it is much hotter than its available(uncertain) spectral type of O7: II-III:. In the case of BI 208, ourinability to fit its observed profiles suggests that its wind is notspherically symmetric. For Sk -67°166, quantitative measurements ofits line strengths confirm the suggestion by Walborn et al. that it is anitrogen-rich O star.Based on observations made with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer. FUSE is operated for NASA by Johns HopkinsUniversity under NASA contract NAS5-32985.
| The relation between radio flux density and ionising ultra-violet flux for HII regions and supernova remnants in the Large Magellanic Cloud
We present a comparison between the Parkes radio surveys (Filipovic etal. 1995) and Vacuum Ultra-Violet (VUV) surveys (Smith et al. 1987) ofthe Large Magellanic Clouds (LMC). We have found 72 sources in common inthe LMC which are known HII regions (52) and supernova remnants (SNRs)(19). Some of these radio sources are associated with two or more UVstellar associations. A comparison of the radio flux densities andionising UV flux for HII regions shows a very good correlation, asexpected from theory. Many of the Magellanic Clouds (MCs) SNRs areembedded in HII regions, so there is also a relation between radio andUV which we attribute to the surrounding HII regions.
| A statistical study of binary and multiple clusters in the LMC
Based on the Bica et al. (\cite{bica}) catalogue, we studied the starcluster system of the LMC and provide a new catalogue of all binary andmultiple cluster candidates found. As a selection criterion we used amaximum separation of 1farcm4 corresponding to 20 pc (assuming adistance modulus of 18.5 mag). We performed Monte Carlo simulations andproduced artificial cluster distributions that we compared with the realone in order to check how many of the found cluster pairs and groups canbe expected statistically due to chance superposition on the plane ofthe sky. We found that, depending on the cluster density, between 56%(bar region) and 12% (outer LMC) of the detected pairs can be explainedstatistically. We studied in detail the properties of the multiplecluster candidates. The binary cluster candidates seem to show atendency to form with components of similar size. When possible, westudied the age structure of the cluster groups and found that themultiple clusters are predominantly young with only a few cluster groupsolder than 300 Myr. The spatial distribution of the cluster pairs andgroups coincides with the distribution of clusters in general; however,old groups or groups with large internal age differences are mainlylocated in the densely populated bar region. Thus, they can easily beexplained as chance superpositions. Our findings show that a formationscenario through tidal capture is not only unlikely due to the lowprobability of close encounters of star clusters, and thus the evenlower probability of tidal capture, but the few groups with largeinternal age differences can easily be explained with projectioneffects. We favour a formation scenario as suggested by Fujimoto &Kumai (\cite{fk}) in which the components of a binary cluster formedtogether and thus should be coeval or have small age differencescompatible with cluster formation time scales. Table 6 is only availablein electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttps://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/391/547
| A CO Survey of the LMC with NANTEN: III. Formation of Stellar Clusters and Evolution of Molecular Clouds
In order to elucidate star formation in the LMC, we made a completestudy of CO clouds with NANTEN. In the present paper, we compare 55giant molecular clouds (GMCs), whose physical quantities were welldetermined, with young objects, such as young stellar clusters and HIIregions. We find that the GMCs are actively forming stars and clusters;23 and 40 are found to be associated with the clusters and the HIIregions, respectively. The clusters associated with the GMCs aresignificantly young; ~ 85% of them are younger than ~ 10 Myr. Inaddition, compact groups of the young clusters are often found at thepeak position of the GMCs, e.g., N 159 and N 44, while much loosergroups are away from the GMCs. This suggests that the clusters areformed in groups and disperse as they become old. The distributions ofthe CO, [CII], and UV indicate that the GMCs are likely to be rapidlydissipated within several Myr due to UV photons from the clusters. Wealso estimate the evolutionary time scale of the GMCs; they form starsin a few Myr after their birth, and form clusters during the next fewMyr, and are dissipated in the subsequent few Myr.
| Lyman Continuum Extinction by Dust in H II Regions of Galaxies
We examine Lyman continuum extinction (LCE) in H II regions by comparinginfrared fluxes of 49 H II regions in the Galaxy, M31, M33, and theLarge Megellanic Cloud with estimated production rates of Lymancontinuum photons. A typical fraction of Lyman continuum photons thatcontribute to hydrogen ionization in the H II regions of three spiralgalaxies is <~50%. The fraction may become smaller as the metallicity(or dust-to-gas ratio) increases. We examine the LCE effect on estimatedstar formation rates of galaxies. The correction factor for the Galacticdust-to-gas ratio is 2-5.
| X-Rays from Superbubbles in the Large Magellanic Cloud. VI. A Sample of Thirteen Superbubbles
We present ROSAT observations and analysis of thirteen superbubbles inthe Large Magellanic Cloud. Eleven of these observations have not beenpreviously reported. We have studied the X-ray morphology of thesuperbubbles and have extracted and analyzed their X-ray spectra.Diffuse X-ray emission is detected from each of these superbubbles, andX-ray emission is brighter than that theoretically expected for awind-blown bubble, suggesting that the X-ray emission from thesuperbubbles has been enhanced by interactions between the superbubbleshell and interior supernova remnants. We have also found significantpositive correlations between the X-ray luminosity of a superbubble andits Hα luminosity, expansion velocity, and OB star count. Further,we have found that a large fraction of the superbubbles in the sampleshow evidence of breakout regions, where hot X-ray-emitting gas extendsbeyond the Hα shell.
| The OB Zoo: A Digital Atlas of Peculiar Spectra
A digital atlas of 20 high-luminosity, peculiar OB spectra in the3800-4900 Å range is presented. The atlas is organized anddiscussed in terms of the following four categories: WN-A or WNL stars,OB Iape or very late WN (WNVL) stars, iron stars, and B-supergiantluminous blue variables (LBVs). Several objects in the earliercategories are also active or quiescent LBVs. Some (but not all) ofthese objects have been well studied, and extensive references areprovided, as are comprehensive spectral-line identifications. Severalnew morphological relationships among the objects have been recognizedthrough this presentation. In particular, attention is drawn to theoccurrence of spatial pairing between nearly identical, unusual spectra,which may have implications for a particular mode of massive-starformation. This small sample includes one or both members of at leastfive such pairs. Physical explanations of these peculiar, likelytransitional spectra and the relationships among them are essential fora complete understanding of massive stellar evolution.
| Ultraviolet Imaging Polarimetry of the Large Magellanic Cloud. II. Models
Motivated by new sounding-rocket wide-field polarimetric images of theLarge Magellanic Cloud (reported simultaneously by Cole et al.), we haveused a three-dimensional Monte Carlo radiation transfer code toinvestigate the escape of near-ultraviolet photons from young stellarassociations embedded within a disk of dusty material (i.e., a galaxy).As photons propagate through the disk, they may be scattered or absorbedby dust. Scattered photons are polarized and tracked until they escapethe dust layer, allowing them to be observed; absorbed photons heat thedust, which radiates isotropically in the far-infrared where the galaxyis optically thin. The code produces four output images: near-UV andfar-IR flux, and near-UV images in the linear Stokes parameters Q and U.From these images we construct simulated UV polarization maps of theLMC. We use these maps to place constraints on the star+dust geometry ofthe LMC and the optical properties of its dust grains. By tuning themodel input parameters to produce maps that match the observedpolarization maps, we derive information about the inclination of theLMC disk to the plane of the sky and about the scattering phase functiong. We compute a grid of models with i=28 deg, 36 deg, and 45 deg, andg=0.64, 0.70, 0.77, 0.83, and 0.90. The model that best reproduces theobserved polarization maps has i=36 deg+2-5 andg~0.7. Because of the low signal-to-noise in the data, we cannot placefirm constraints on the value of g. The highly inclined models do notmatch the observed centrosymmetric polarization patterns around brightOB associations or the distribution of polarization values. Our modelsapproximately reproduce the observed ultraviolet photopolarimetry of thewestern side of the LMC; however, the output images depend on many inputparameters and are nonunique. We discuss some of the limitations of themodels and outline future steps to be taken; our models make somepredictions regarding the polarization properties of diffuse lightacross the rest of the LMC.
| The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud
The catalogue provides for each of the 134 W-R stars of Population Ipresently known in the Large Magellanic Cloud, accurate equatorialcoordinates, photometric data, spectral classification, binary status,correlation with OB associations and HII regions. The miscellaneousdesignations of the stars are also listed. Although completeness is notpretended, results published during the last decade are highlighted inthe notes given for each individual star. A uniform set of findingcharts is presented. Figures 2 to 12 only in the electronic version athttps://edpsciences.com
| A Revised and Extended Catalog of Magellanic System Clusters, Associations, and Emission Nebulae. II. The Large Magellanic Cloud
A survey of extended objects in the Large Magellanic Cloud was carriedout on the ESO/SERC R and J Sky Survey Atlases, checking entries inprevious catalogs and searching for new objects. The census provided6659 objects including star clusters, emission-free associations, andobjects related to emission nebulae. Each of these classes containsthree subclasses with intermediate properties, which are used to infertotal populations. The survey includes cross identifications amongcatalogs, and we present 3246 new objects. We provide accuratepositions, classification, and homogeneous measurements of sizes andposition angles, as well as information on cluster pairs andhierarchical relation for superimposed objects. This unification andenlargement of catalogs is important for future searches of fainter andsmaller new objects. We discuss the angular and size distributions ofthe objects of the different classes. The angular distributions show twooff-centered systems with different inclinations, suggesting that theLMC disk is warped. The present catalog together with its previouscounterpart for the SMC and the inter-Cloud region provide a totalpopulation of 7847 extended objects in the Magellanic System. Theangular distribution of the ensemble reveals important clues on theinteraction between the LMC and SMC.
| Ultraviolet observations of stars in the Magellanic Clouds: a historical bridge from the Sun to R 136 and beyond.
Not Available
| Young clusters in the Magellanics Clouds.
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| Ultraviolet Imaging Telescope Observations of the Magellanic Clouds
We present wide-field far-ultraviolet (FUV; 1300-1800 Å) images ofthe Large and Small Magellanic Clouds (LMC, SMC). These data wereobtained by the Ultraviolet Imaging Telescope (UIT) during the Astro-1(1990 December 1-10) and Astro-2 (1995 March 2-18) missions; the imagesprovide an extensive FUV mosaic of the SMC and contain numerous regionsin the LMC, covering a wide range of stellar densities and current starformation activity. A total of 47 LMC/Lucke-Hodge and 37 SMC/Hodge OBassociations are completely or partially included in the observedfields. FUV data can identify the hottest OB stars more easily than canoptical photometry, and these stars dominate the ionizing flux, which iscorrelated to the observed Hα flux of the associated H ii regions.Of the H ii regions in the catalog of Davies, Elliott, & Meaburn(DEM), the UIT fields completely or partially include 102 DEM regions inthe LMC and 74 DEM regions in the SMC. We present a catalog of FUVmagnitudes derived from point-spread function photometry for 37,333stars in the LMC (the UIT FUV magnitudes for 11,306 stars in the SMCwere presented recently by Cornett et al.), with a completeness limit ofm_UV ~ 15 mag and a detection limit of m_UV ~ 17.5. The averageuncertainty in the photometry is ~0.1 mag. The full catalog withastrometric positions, photometry, and other information is alsoavailable from publicly accessible astronomical data archives. We dividethe catalog into field stars and stars that are in DEM regions. Weanalyze each of these two sets of stars independently, comparing thecomposite UV luminosity function of our data with UV magnitudes derivedfrom stellar evolution and atmosphere models in order to derive theunderlying stellar formation parameters. We find a most probable initialmass function (IMF) slope for the LMC field stars of Gamma = -1.80 +/-0.09. The statistical significance of this single slope for the LMCfield stars is extremely high, though we also find some evidence for afield star IMF slope of Gamma ~ -1.4, roughly equal to the Salpeterslope. However, in the case of the stars in the DEM regions (the starsin all the regions were analyzed together as a single group), we findthree IMF slopes of roughly equal likelihood: Gamma = -1.0, -1.6, and-2.0. No typical age for the field stars is found in our data for timeperiods up to a continuous star formation age of 500 Myr, which is themaximum age consistent with the completeness limit magnitude of thecatalog's luminosity function. The best age for the collection ofcluster stars was found to be t_0 = 3.4 +/- 1.9 Myr; this is consistentwith the age expected for a collection of OB stars from many differentclusters.
| Evolutionary status and age spread in the young LMC cluster NGC 1850A
IUE spectra have been obtained for 15 members of the very young LMCcluster NGC 1850A. The extinction law toward the cluster is similar tothe one generally accepted for the 30 Dor region. We derive theeffective temperatures and bolometric luminosities to estimate the ageand mass for each star. An age spread of 2 to 10 Myr is estimated,suggesting a more or less continuous star formation process. The clustercontains at least four objects with mass >= 55 M_sun, still close tothe main sequence. The age of the main cluster NGC 1850 is estimated tobe about 50 Myr. Based on observations collected by the InternationalUltraviolet Explorer (IUE) at the Villafranca Satellite Tracking Stationof the European Space Agency.
| Scaleheights of 486 southern spiral galaxies and some statistical correlation
Based on Peng's method (1988), we obtain scaleheights of 486 southernspiral galaxies, the images of which are taken from the Digitized SkySurvey at Xinglong Station of Beijing Astronomical Observatory. Thefitted spiral arms of 70 galaxies are compared with their images to gettheir optimum inclinations. The scaleheights of other 416 ones arelisted in Table A1 in Appendix. After compiling and analyzing the data,we find some statistical correlations. The most interesting results arethat a flatter galaxy is bluer and looks brighter, and galaxies becomeflatter along the Hubble sequence Sab -- Scd. Based on photographic dataof the National Geographic Society -- Palomar Observatory Sky Survey(NGS-POSS) obtained using the Oschin Telescope Palomar Mountain. TheNGS-POSS was funded by a grant from the National Geographic Society tothe California Institute of Technology. The plates were processed intothe present compressed digital form with their permission. The DigitizedSky Survey was produced at the Space Telescope Science Institute underUS Government grant NAG W-2166. Table A1 is available in electronic fromonly, via anonymous ftp 130.79.128.5 orhttps://cdsweb.u-strasbg.fr/Abstract.html
| H_2 and its relation to CO in the LMC and other magellanic irregular galaxies
H_2 column densities towards CO clouds in the LMC and SMC are estimatedfrom their far-infrared surface brightness and HI column density. Thenewly derived H_2 column densities imply N(H_{2)}/I(CO) conversionfactors (in units of 10(21) mol cm(-2) (K km s(-1) )(-1) ) X_LMC =1.3+/-0.2 and X_SMC = 12+/-2. LMC and SMC contain total (warm) H_2masses of 1.0+/-0.3 x 10(8) Msun and 0.75+/-0.25 x 10(8)Msun respectively. Local H_2/HI mass ratios similar to thosein LMC and SMC are found in the magellanic irregulars NGC 55, 1569,4214, 4449 and 6822 and in the extragalactic HII region complexes NGC604, 595 and 5461 in M 33 and M 101 respectively. In these HII regionsand in NGC 4449, we find X = 1-2; in NGC 55, 4214 and 6822 X = 3-6 againin units of 10(21) mol cm(-2) (K km s(-1) )(-1) . The post-starburstgalaxy NGC 1569 has a very high value similar to that of the SMC. TheCO-H_2 conversion factor X is found to depend on both the ambientradiation field intensity per nucleon {sigma _FIR/{N_H and metallicity[O]/[H]: log X ~ 0.9+/-0.1 logfrac {sigma _FIR{N_H - 3.5+/-0.2log([O])/([H]). Neglecting dependency on radiation field, a reasonableapproximation is also provided by log X ~ -2.7+/-0.3 log([O])/([H]).Milky Way values are consistent with these relations. This result isinterpreted as the consequence of selective photodissociation of COsubjected to high radiation field energy densities and poor(self)shielding in low-metallicity environments, and especially thepreferential destruction of diffuse CO in `interclump' gas. Althoughlocally H_2 may be the dominant ISM-component, the average global H_2/HImass ratio is 0.2+/-0.04 and the average H_2 gas mass fraction is0.12+/-0.02. Magellanic irregulars have warm molecular gas fractionsvery similar to those of our Galaxy, whereas other global properties(mass, luminosity, metallicity, CO luminosity) are very different.
| No stellar age gradient inside supergiant shell LMC4
The youngest stellar populations of a 'J'-shaped region inside thesupergiant shell (SGS) LMC4 have been analysed with CCD photometry in B,V passbands. This region consists of 2 coherent strips, one from theeast to the west reaching about 400;pc across the OB superassociationLH77 and another extending about 850;pc from south to north. Thestandard photometric methods yield 25 colour-magnitude diagrams (CMDs)which were used for age determination of the youngest star population byisochrone fitting. The resultant ages lie in the range from 9;Myr to16;Myr without correlation with the distance to the LMC4 centre. Wetherefore conclude that there must have been one triggering event forstar formation inside this great LMC SGS with a diameter of 1.4;kpc. Weconstruct the luminosity function and the mass function of five regionsconsisting of 5 fields to ensure that projection effects don't mask theresults. The slopes lie in the expected range (gamma in [0.22;0.41] andGamma in [-1.3;-2.4] respectively). The greatest values of the slopeoccur in the north, which is caused by the absence of a young,number-dominating star population. We have calculated the rate withwhich supernovae (SNe) have exploded in LMC4, based on the finding thatall stars are essentially coeval. A total of 5--7*10(3) supernovae hasdumped the energy of 10(54.5) ;erg over the past 10;Myr into LMC4, infact enough to tear the original star-forming cloud apart in the timespan between 5 and 8;Myr after the starformation burst. We conclude thatLMC4 can have been formed without a contribution from stochasticself-propagating star formation (SSPSF), although the ring of youngassociations and HiI\ regions around the edge have been triggered by theevents inside LMC4. Based on observations collected at the EuropeanSouthern Observatory (ESO), La Silla, Chile.
| Supernova Remnants in OB Associations
Abstract image available at:https://adsabs.harvard.edu/abs/1997AJ....113.1815C
| LH 72, the Center of Constellation III
Ultraviolet spectroscopy with IUE is combined with optical photometry tostudy the brightest blue members of the LMC OB association LH 72. LH 72lies near the geometric center of Shapley's Constellation III, a complexof gas and stars that makes up one of the largest known superbubbles.Ages for the stars range from 5 x 106 to 1.5 x 107 yr, with agesincreasing from the south to the north end of the association. Theyoungest stars are associated with the brightest H II emission and havethe largest reddening. This pattern of apparent sequential starformation is contrary to the expanding model proposed by Dopita,Mathewson, & Ford, in which the entire superbubble, more than anorder of magnitude larger in size than LH 72, evolves in about the sameamount of time. Our data, however, are consistent with an alternativemodel (Reid, Mould, & Thompson), in which star formation proceedslocally after the initial trigger from the superbubble shock.
| IUE Observations of Young Clusters in the Large Magellanic Cloud
Abstract image available at:https://adsabs.harvard.edu/abs/1996ApJ...458..580W
| Integrated UBV Photometry of 624 Star Clusters and Associations in the Large Magellanic Cloud
We present a catalog of integrated UBV photometry of 504 star clustersand 120 stellar associations in the LMC, part of them still embedded inemitting gas. We study age groups in terms of equivalent SWB typesderived from the (U-B) X (B-V) diagram. The size of the spatialdistributions increases steadily with age (SWB types), whereas adifference of axial ratio exists between the groups younger than 30 Myrand those older, which implies a nearly face-on orientation for theformer and a tilt of ~45^deg^ for the latter groups. Asymmetries arepresent in the spatial distributions, which, together with thenoncoincidence of the centroids for different age groups, suggest thatthe LMC disk was severely perturbed in the past.
| Ultraviolet spectral evolution of star clusters in the IUE library.
The ultraviolet integrated spectra of star clusters and H II regions inthe IUE library have been classified into groups based on their spectralappearance, as well as on age and metallicity information from otherstudies. We have coadded the spectra in these groups according to theirS/N ratio, creating a library of template spectra for futureapplications in population syntheses in galaxies. We define spectralwindows for equivalent width measurements and for continuum tracings.These measurements in the spectra of the templates are studied as afunction of age and metallicity. We indicate the windows with a strongmetallicity dependence, at different age stages.
| Extinction characteristics of giant HII regions - Star-forming complexes in the galaxies M33, LMC, and NGC 2403
The discrepancies between the extinction of gas emission and that of thestarlight in giant HII regions, star-forming complexes in the galaxiesM33, LMC, and NGC 2403, were empirically investigated. The extinctionvalues were determined for 30 stars in eight associations in M33. Anempirical relation between the extinction of starlight and that of thegas emission in giant HII regions, star-forming complexes in thegalaxies under study, was obtained.
| A radio continuum study of the Magellanic Clouds. IV. Catalogues of radio sources in the Large Magellanic Cloud at 1.40, 2.45, 4.75, 4.85 and 8.55 GHz.
From observations with the Parkes radio telescope, we present cataloguesof radio sources in the Large Magellanic Cloud at four frequencies:1.40, 2.45, 4.75 and 8.55GHz, and an additional catalogue from a sourceanalysis of the Parkes-MIT-NRAO survey at 4.85GHz. A total of 469sources have been detected at least one of these frequencies, 132 ofwhich are reported here for the first time as radio sources.
| Ultraviolet interstellar absorption lines in the LMC: Searching for hidden SNRs
Strong x-ray emission detected in Large Magellanic Cloud (LMC)superbubbles has been explained as the result of interior supernovaremnants (SNRs) hitting the dense superbubble shell. Such SNRs cannot befound using conventional criteria. We thus investigate the possibilityof using the interstellar absorption properties in the ultraviolet (UV)as a diagnostic of hidden SNR shocks. The International UltravioletExplorer (IUE) archives provide the database for this pilot study. Theycontain high-dispersion spectra of several stars in x-ray brightsuperbubbles. To distinguish the effects of SNR shocks from those oflocal stellar winds and a global hot halo around the LMC, we includedcontrol objects in different environments. We find that almost allinterstellar absorption properties can be explained by the interstellarenvironment associated with the objects. Summarizing the two mostimportant results of this study: (1) a large velocity shift between thehigh-ionization species (C IV and Si IV) and the low-ionization species(S II, Si II, and C II*) is a diagnostic of hidden SNR shocks; however,the absence of a velocity shift does not preclude the existence of SNRshocks; (2) there is no evidence that the LMC is uniformly surrounded byhot gas; hot gas is preferentially found associated with largeinterstellar structures like superbubbles and supergiant shells, whichmay extend to large distances from the plane.
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